The gas release rate in the belt of the \(\beta \)  Pic system could be up to 0.1 M\(_\oplus \) /Myr [1]} but we note that the gas release rate necessary to explain the CO mass observed could be lower, as there could be sufficient carbon to shield CO from photodissociation in this system [2]}. The temperature conditions of planetesimals in the KB could be similar to that of other exo-Kuiper belts, as belts tend to form preferentially at a given distance from their star [3]}, and so the resulting belt temperature (\(\propto L_\star ^{0.16}\) ) is only weakly dependent on the stellar luminosity (56 K for the \(\beta \)  Pic extrapolation) and close to that of the KB.
We note that the size distribution in young systems could be different to that of the Solar System, which could also increase/decrease the model predictions but this is not taken into account here. A more thorough study (including collisions for young systems) of this model (and its free parameters such as the material composition or temperature of the belt) and whether it can explain all observations (or just that of the less massive belts for instance) is beyond the scope of this KB-focused paper.
